Wolf-Rayet (WR) stars are understood to have clumpy winds [1]. Robert et al. [2] found a statistical relation between the variations of the polarization and the scattering light intensity, R = σ p/σ phot ≈ 0.05. To explain this result, we propose a model in which clumps are ejected from the surface of WR stars uniformly in space with a Gaussian time interval distribution. According to the observed R along with the subpeaks on the emission lines of WR stars, we can obtain the parameters of the velocity law index β, and of the clump ejection rate in a flow time N. Also, the fraction η of the total mass loss rate contained in the clumps can be found from the observed polarization.
| Identifer | oai:union.ndltd.org:ETSU/oai:dc.etsu.edu:etsu-works-17316 |
| Date | 29 May 2012 |
| Creators | Li, Q., Cassinelli, J. P., Brown, J. C., Ignace, Richard |
| Publisher | Digital Commons @ East Tennessee State University |
| Source Sets | East Tennessee State University |
| Detected Language | English |
| Type | text |
| Source | ETSU Faculty Works |
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